scholarly journals Inference on Gravitational Waves from Coalescences of Stellar-Mass Compact Objects and Intermediate-Mass Black Holes

2017 ◽  
pp. 55-72
Author(s):  
Carl-Johan Haster
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Stellar Mass ◽  
Compact Objects ◽  
Intermediate Mass ◽  
Intermediate Mass Black Holes

scholarly journals Inference on gravitational waves from coalescences of stellar-mass compact objects and intermediate-mass black holes

2016 ◽  
Vol 457 (4) ◽  
pp. 4499-4506 ◽  
Author(s):  
Carl-Johan Haster ◽  
Zhilu Wang ◽  
Christopher P. L. Berry ◽  
Simon Stevenson ◽  
John Veitch ◽  
...  
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Stellar Mass ◽  
Compact Objects ◽  
Intermediate Mass ◽  
Intermediate Mass Black Holes

scholarly journals mocca-survey Database I: Binary black hole mergers from globular clusters with intermediate mass black holes

2020 ◽  
Vol 498 (3) ◽  
pp. 4287-4294
Author(s):  
Jongsuk Hong ◽  
Abbas Askar ◽  
Mirek Giersz ◽  
Arkadiusz Hypki ◽  
Suk-Jin Yoon
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Waves ◽  
Globular Clusters ◽  
Stellar Mass ◽  
Intermediate Mass ◽  
Binary Black Holes ◽  
Black Hole Binaries ◽  
Binary Black Hole ◽  
Intermediate Mass Black Holes

ABSTRACT The dynamical formation of black hole binaries in globular clusters that merge due to gravitational waves occurs more frequently in higher stellar density. Meanwhile, the probability to form intermediate mass black holes (IMBHs) also increases with the density. To explore the impact of the formation and growth of IMBHs on the population of stellar mass black hole binaries from globular clusters, we analyse the existing large survey of Monte Carlo globular cluster simulation data (mocca-survey Database I). We show that the number of binary black hole mergers agrees with the prediction based on clusters’ initial properties when the IMBH mass is not massive enough or the IMBH seed forms at a later time. However, binary black hole formation and subsequent merger events are significantly reduced compared to the prediction when the present-day IMBH mass is more massive than ${\sim}10^4\, \rm M_{\odot }$ or the present-day IMBH mass exceeds about 1 per cent of cluster’s initial total mass. By examining the maximum black hole mass in the system at the moment of black hole binary escaping, we find that ∼90 per cent of the merging binary black holes escape before the formation and growth of the IMBH. Furthermore, large fraction of stellar mass black holes are merged into the IMBH or escape as single black holes from globular clusters in cases of massive IMBHs, which can lead to the significant underpopulation of binary black holes merging with gravitational waves by a factor of 2 depending on the clusters’ initial distributions.

scholarly journals On the coexistence of stellar-mass and intermediate-mass black holes in globular clusters

2014 ◽  
Vol 444 (1) ◽  
pp. 29-42 ◽  
Author(s):  
Nathan W. C. Leigh ◽  
Nora Lützgendorf ◽  
Aaron M. Geller ◽  
Thomas J. Maccarone ◽  
Craig Heinke ◽  
...  
Keyword(s):  
Black Holes ◽  
Globular Clusters ◽  
Stellar Mass ◽  
Intermediate Mass ◽  
Intermediate Mass Black Holes

scholarly journals GRAVITATIONAL WAVES FROM INTERMEDIATE-MASS BLACK HOLES IN YOUNG CLUSTERS

2010 ◽  
Vol 719 (2) ◽  
pp. 987-995 ◽  
Author(s):  
M. Mapelli ◽  
C. Huwyler ◽  
L. Mayer ◽  
Ph. Jetzer ◽  
A. Vecchio
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Intermediate Mass ◽  
Young Clusters ◽  
Intermediate Mass Black Holes

Do Intermediate-Mass Black Holes Exist?

2014 ◽  
Author(s):  
Charles D. Bailyn
Keyword(s):  
Black Holes ◽  
Empirical Evidence ◽  
Stellar Mass ◽  
Supermassive Black Holes ◽  
The Sun ◽  
Intermediate Mass ◽  
Lines Of Evidence ◽  
Intermediate Mass Black Holes

This chapter addresses the existence of intermediate-mass black holes. There is powerful empirical evidence for two classes of black holes, namely, the stellar-mass black holes, with masses a few times that of the Sun, and the supermassive black holes at the centers of galaxies. The considerable gap in mass between these two categories naturally prompts the question whether black holes might exist at other mass scales. In recent years, two lines of evidence have been presented in support of the idea that black holes with masses intermediate between stellar mass and supermassive might exist. Such sources are referred to as intermediate-mass black holes. In both cases the results are currently still ambiguous, and much debated.

scholarly journals Detecting Kozai–Lidov Imprints on the Gravitational Waves of Intermediate-mass Black Holes in Galactic Nuclei

2020 ◽  
Vol 901 (2) ◽  
pp. 125 ◽  
Author(s):  
Barnabás Deme ◽  
Bao-Minh Hoang ◽  
Smadar Naoz ◽  
Bence Kocsis
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Galactic Nuclei ◽  
Intermediate Mass ◽  
Intermediate Mass Black Holes

Gravitational Waves from Merging Intermediate‐Mass Black Holes

2004 ◽  
Vol 614 (2) ◽  
pp. 864-868 ◽  
Author(s):  
Tatsushi Matsubayashi ◽  
Hisa‐aki Shinkai ◽  
Toshikazu Ebisuzaki
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Intermediate Mass ◽  
Intermediate Mass Black Holes

scholarly journals Gravitational Waves from Merging Intermediate-Mass Black-Holes

2004 ◽  
Vol 155 ◽  
pp. 415-416 ◽  
Author(s):  
Tatsushi Matsubayashi ◽  
Hisa-aki Shinkai ◽  
Toshikazu Ebisuzaki
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Intermediate Mass ◽  
Intermediate Mass Black Holes

scholarly journals Observing Intermediate-mass Black Holes and the Upper Stellar-mass gap with LIGO and Virgo

2022 ◽  
Vol 924 (1) ◽  
pp. 39
Author(s):  
Ajit Kumar Mehta ◽  
Alessandra Buonanno ◽  
Jonathan Gair ◽  
M. Coleman Miller ◽  
Ebraheem Farag ◽  
...  
Keyword(s):  
Black Holes ◽  
Reaction Rate ◽  
Signal To Noise Ratio ◽  
Mass Range ◽  
Mass Function ◽  
Stellar Mass ◽  
Intermediate Mass ◽  
Mass Gap ◽  
Model Finding ◽  
Intermediate Mass Black Holes

Abstract Using ground-based gravitational-wave detectors, we probe the mass function of intermediate-mass black holes (IMBHs) wherein we also include BHs in the upper mass gap at ∼60–130 M ⊙. Employing the projected sensitivity of the upcoming LIGO and Virgo fourth observing run (O4), we perform Bayesian analysis on quasi-circular nonprecessing, spinning IMBH binaries (IMBHBs) with total masses 50–500 M ⊙, mass ratios 1.25, 4, and 10, and dimensionless spins up to 0.95, and estimate the precision with which the source-frame parameters can be measured. We find that, at 2σ, the mass of the heavier component of IMBHBs can be constrained with an uncertainty of ∼10%–40% at a signal-to-noise ratio of 20. Focusing on the stellar-mass gap with new tabulations of the 12C(α, γ)16O reaction rate and its uncertainties, we evolve massive helium core stars using MESA to establish the lower and upper edges of the mass gap as ≃ 59 − 13 + 34 M ⊙ and ≃ 139 − 14 + 30 M ⊙ respectively, where the error bars give the mass range that follows from the ±3σ uncertainty in the 12C(α, γ)16O nuclear reaction rate. We find that high resolution of the tabulated reaction rate and fine temporal resolution are necessary to resolve the peak of the BH mass spectrum. We then study IMBHBs with components lying in the mass gap and show that the O4 run will be able to robustly identify most such systems. Finally, we reanalyze GW190521 with a state-of-the-art aligned-spin waveform model, finding that the primary mass lies in the mass gap with 90% credibility.

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